Visible Spectrum

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Wein’s Law• As the temperature goes up there are more collisions & more violent• So more photons AND more energetic photons• Higher temperature shorter wavelength of peak emission=• Higher temperature bluer color
Stefan-Boltzmann Law• E= σ T 4• The amount of energy radiated is proportional totemperature to the fourth power• Twice the temperature give 2X2X2x2=16 times the energy
Page 1 and 2: Visible Spectrum• Prism splits Vi
Page 3 and 4: Electromagnetism• Changing electr
Page 5 and 6: All Electromagnetic WavesMove at th
Page 7 and 8: Radio Waves• Hertz discovered rad
Page 9: Infrared Region• Bag is transpare
Page 12 and 13: Gamma Rays• Produced by very hot
Page 14 and 15: Atmospheric Opacity• Opacity is t
Page 16 and 17: Heat or Thermal Energy• The hotte
Page 18 and 19: Blackbody Radiation• A blackbody
Page 22 and 23: Blackbody Curve• After attempts b
Page 24 and 25: Planet Impact?• Star HD172555 has
Page 26 and 27: Moving Source• Wavelengths in dir
Page 28 and 29: Relative Motion• Stationary obser
Page 30 and 31: Picturesof Atoms• 48 iron atoms o
Page 32 and 33: What’s an Atom?-Nucleus & Electro
Page 34 and 35: Neutrons & Isotopes
Page 37 and 38: Bohr Atom• Tiny positive nucleusc
Page 39 and 40: Photon Emission/Absorption• The e
Page 41 and 42: Electron: is a particle & a wave•
Page 43 and 44: EmissionMatchesAbsorptionSpectrum
Page 45 and 46: PhotonAbsorptionandEmission• Elec
Page 47 and 48: Spectra ofMolecules• Carbon Monox
Page 49 and 50: Annie Jump Cannon• Originated the
Page 51 and 52: Cecilia Payne-Gaposchkin• Found t
Page 53 and 54: Thermal Broadening• Because the a
Page 55 and 56: Pressure/Collisional Broadening•
Page 57 and 58: Discovering Extrasolar Planets• S
Page 60 and 61: Electromagnetic Spectrum• All ele
Page 62 and 63: Energy LevelDiagram of aHydrogen At
Page 64 and 65: Pressure• Gas is made of tiny ato
Page 66 and 67: Relative Radii of Atoms• Atomic r
Page 68 and 69: Time to Solar System Formation• M
Page 70 and 71:
Transitions of Hydrogen• Differen
Page 72 and 73:
Spectral Sequence = Temperature Seq
Page 74 and 75:
Solar Spectrum• Millions of absor
Page 76 and 77:
Types of SpectraWe usually look at
Page 78 and 79:
(B-V) Color Index• Counting the n
Page 80 and 81:
Wien’s Law• Wavelength of maxim
Page 82 and 83:
Loss ofAtmosphere• First atmosphe
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Visible Spectrum

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